Lecture 4.E. Modeling Stellar Absorption

In this Lecture we cover the convolution of the Lorenztians of natural and pressure broadening, and the Gaussians of thermal and turbulent broadening to yield the Voigt function. We then cover rotational broadening. We end absorption line modeling with the convolution of the instrumental spread profile. We close by very briefly discussing the continuum opacity in stars, especially neutral H, the H- ion and electron scattering.